Upload
others
View
10
Download
0
Embed Size (px)
Citation preview
PAMELA SPACE MISSIONPAMELA SPACE MISSION
Piergiorgio PicozzaPamela Collaboration
INFN & University of Roma “Tor Vergata”
XII International Workshop XII International Workshop on Neutrino Telescopeson Neutrino Telescopes
VeniceVenice, , ItalyItaly
6 6 –– 9 9 MarchMarch 20072007
PAMELAPAMELAPPayload for ayload for AAntimatter ntimatter
MMatter atter EExploration and xploration and LLight Nucleiight Nuclei AAstrophysicsstrophysics
LaunchedLaunched in in orbitorbit on on JuneJune 15, 2006, on 15, 2006, on board of the DK1 satellite board of the DK1 satellite byby a a SoyuzSoyuzrocketrocket fromfrom the Bajkonour launch site.the Bajkonour launch site.
SinceSince July 11, 2006, Pamela is in July 11, 2006, Pamela is in continuouscontinuous data data takingtaking modemode
Bari Florence Frascati
Italy:TriesteNaples Rome CNR, Florence
MoscowSt. Petersburg
Russia:
Germany:Siegen
Sweden:KTH, Stockholm
PAMELA CollaborationPAMELA Collaboration
WiZardWiZard RussianRussian ItalianItalian MissionsMissions
…1989 · 1990 · 1991 · 1992 · 1993 · 1994 · 1995 · 1996 · 1997 · 1998 · 1999 · 2000 · 2001 · 2002 · 2003 · 2004 · 2005 · 2006 · 2007..
PAMELA
NINA-1 NINA-2SILEYE-1
SILEYE-2
Alteino-SILEYE-3
ALTEA-SILEYE-4
•M 89
•M 91
•TS 93
•C 94
•C 97
•C 98
SILEYE-2 SILEYE-1 ALTEINO: SILEYE-3 ALTEA:
SILEYE-4LAZIO SIRAD
MASS-89, 91, TS-93, CAPRICE 94-97-98
NINA-2NINA-1 PAMELA
The PAMELA The PAMELA InstrumentInstrument
GFGF ~21.5 cm~21.5 cm22srsrMass: 470 kgMass: 470 kgSizeSize: 120x70x70 cm: 120x70x70 cm33
Power Budget: 360 WPower Budget: 360 W
Mass&Thermal ModelFull cycle of vibration/shock/ tranporttests
Technological ModelPreliminaryAcceptance Tests withEGSE: power ON/OFF, telecommands, data transmission
Flight ModelIntegration, beam tests;pre-flight operations
PAMELA MODELS
PAMELA InstrumentPAMELA Instrument
Shower tail catcherShower tail catcherScintillatorScintillator
ToFToF
Magnetic Magnetic spectrometerspectrometer
CalorimeterCalorimeter
AnticoincidenceAnticoincidenceshieldshield
Neutron DetectorNeutron Detector
MAGNETIC SPECTROMETERB=0.48T Nd-B-Fe6 planes double sided Si strips 300 μm thickSpatial resolution ~3μmMDR = 1 TV/c
TOFFirst level trigger Particle identification(up to 1GeV/c)dE/dx
IMAGING CALORIMETER44 Si layers intervealed with 22 W planes 16.3 X0 / 0.6 l0e+/p and p/e- at level of 10-4
~ 10-5
SHOWER TAIL CATCHER SCINTILLATOR
•Neutron Detector Trigger
NEUTRON DETECTOR36 3He counters in polyetilenmoderators to discriminate between very high energyelectron and protoncomponents
ANTICOINCIDENCE SHIELD
• Scintillator paddles 10 mm thick
•Dynamic range of 1÷1000 mip
GF: 21.5 cm2 sr Mass: 470 kgSize: 130x70x70 cm3
Power Budget: 360W
PAMELA nominal capabilitiesPAMELA nominal capabilitiesenergyenergy rangerange particlesparticles in in 3 y3 yeaearrss
Antiprotons Antiprotons 80 80 MeVMeV -- 190 190 GeVGeV ~ 10~ 1044
Positrons Positrons 50 50 MeVMeV –– 270 270 GeVGeV ~ 10~ 1055
Electrons Electrons up to 400 up to 400 GeVGeV ~ 10~ 1066
Protons Protons up to 700 up to 700 GeVGeV ~ 10~ 1088
Electrons+positronsElectrons+positrons up to 2 up to 2 TeVTeV (from calorimeter)(from calorimeter)
Light NucleiLight Nuclei up to 200 up to 200 GeV/nGeV/n He/Be/C: ~10He/Be/C: ~107/4/57/4/5
AntiNucleiAntiNuclei searchsearch sensitivity of sensitivity of 3x3x1010--88 in in antiHeantiHe/He/He
Orbit Characteristics
70.4ο
610 km
350 kmSAA
• Low-earth elliptical orbit
• 350 – 610 km
• Quasi-polar (70o inclination)
• Lifetime >3 years (assisted)
• Radiation Belts - SAA
• Geomagnetic cutoff
Ground Station(s)MainMain Station:Station: Research Centre for Earth Operative Monitoring Research Centre for Earth Operative Monitoring
““NtsOMZNtsOMZ”” ((MoscowMoscow, Russia);, Russia);
Main antenna in NTsOMZ
Scheme of PAMELA control room in NTsOMZ
PAMELA statusPAMELA statusFirst switchFirst switch--on on June 21on on June 21stst 20062006
•• Detectors in nominal conditions (no problems due to the launch)Detectors in nominal conditions (no problems due to the launch)•• Tested different trigger and hardware configurationsTested different trigger and hardware configurations•• Commissioning phase successfully ended on July 11Commissioning phase successfully ended on July 11thth 20062006
PAMELA in continuous dataPAMELA in continuous data--taking modetaking mode
16 Gigabytes of Data daily 16 Gigabytes of Data daily trasmittedtrasmitted to Groundto Ground
At January 30At January 30thth 2007:2007:PAMELA ON for 201 daysPAMELA ON for 201 days20880 acquisition runs20880 acquisition runs2.8 TB of raw data 2.8 TB of raw data 344961274 triggers recorded344961274 triggers recorded
Remote controlRemote control
MacrocommandsMacrocommands: commands to PAMELA : commands to PAMELA cpucpuSystem configuration (hundreds of modifiable System configuration (hundreds of modifiable parameters):parameters):Calibration (ascending node)Calibration (ascending node)Download to satellite mass memoryDownload to satellite mass memory……
TelecommandsTelecommands: hardware lines to handle power : hardware lines to handle power modulesmodules
Extremely flexible system, designed to be easily Extremely flexible system, designed to be easily adapted to space (unknown) conditions.adapted to space (unknown) conditions.
Download @orbit 3754 – 15/02/2007 07:35:00 MWT
S1
S2S3
Inner radiation belt
(SSA)
orbit 3752 orbit 3753orbit 3751
NP SP
EQ EQ
Outer radiation belt
95 min
Another possible scenario: KK Dark Matter
Lightest Kaluza-Klein Particle (LKP): B(1)
Bosonic Dark Matter:fermionic final states no longer helicity suppressed.e+e- final states directly produced.
As in the neutralino case there are 1-loopprocesses that produces monoenergeticγ γ in the final state.
Search of structures in antiproton spectrum
Secondary production(upper and lower limits)Simon et al.
Secondary production(CAPRICE94-based)Bergström et al.
Primary production from χχ annihilation (m(χ) = ~ 1 TeV)
( astro-ph 9904086)
Distortion of the secondary positron fraction induced by a signaDistortion of the secondary positron fraction induced by a signal from a heavy l from a heavy neutralinoneutralino..
Baltz & EdsjöPhys.Rev. D59 (1999)astro-ph 9808243
Antiproton spectra: Antiproton spectra: Pamela expectation forPamela expectation for
Diffuse and Convection model in 3 yearDiffuse and Convection model in 3 year
Antiproton spectra: PAMELA expectation for DC model
A.Lionetto, A.Morselli, V.Zdravkovic, JCAP09(2005)010
Propagation Equation for Cosmic Rays in the Milky Way Propagation Equation for Cosmic Rays in the Milky Way
convection velocity field that corresponds to galactic wind and it has a cylindrical symmetry, as the geometry of the galaxy. It’s z-component is the only one different from zero and increases linearly with the distance from the galactic plane
loss term: fragmentationloss term: radioactive decay
diffusion coefficient is function of rigidity
diffusion coefficient in the impulse space,quasi-linear MHD:
primary spectra injection index
implemented in Galprop (Strong & Moskalenko, available on the Web)
Comparison of p/p ratio with modelTime variation of p/p ratio at solar maximum
Observed data by BESS
Charge dependent model
prediction(Bieber et al.)
Charge dependent solar modulation model well follows
the suddenly increase of p/pratio observed by BESS
at the solar polarity reversal between 1999 and 2000
Comparison of p/p ratio with modelTime variation of p/p ratio at solar maximum
Observed data by BESS
Charge dependent model
prediction(Bieber et al.)
Charge dependent solar modulation model well follows
the suddenly increase of p/pratio observed by BESS
at the solar polarity reversal between 1999 and 2000
Impulsive event13/12/2006
CME already on 6/12
Pamela ON before and at onset of event
Time division:Before shock (3UTC)
During shock before Memory fill(3UTC-4.55UTC)
After Memory download (11:15-12.55UTC)
Plot of the particle rate at 10 MIP threshold in Normal mode for the period of days ranging from 12/11/2006 to 12/14/2006. This period of time includes a Solar Flare event revealing its presence with an abrupt rate increasing in correspondence of December the 13th.
–– High energy from ~ 1 High energy from ~ 1 GeVGeV to ~ 10 to ~ 10 GeVGeV
–– Content of eContent of e++, e, e--, p, 3He, p, 3He
–– Low LLow L-- shell shell ⇔⇔ low altitudelow altitude
–– Life time Life time O(secondsO(seconds))
⇒⇒ Secondary production from CR interactionSecondary production from CR interactionwith atmospherewith atmosphere
High Energy Radiation Belts
High High EnergyEnergy electronselectrons
The study of primary electrons is especially important because they give information on the nearest sources of cosmic rays
Electrons with energy above 100 MeV rapidly loss their energy due to synchrotron radiation and inverse Compton processes
The discovery of primary electrons with energy above 1012 eV will evidence the existence of cosmic ray sources in the nearby interstellar space (r≤300 pc)
EarliestEarliest exampleexample of the interplay of the interplay betweenbetweenparticlesparticles physicsphysics and and cosmologycosmology
““WeWe mustmust regardregard itit ratherrather anan accidentaccident thatthat the the EarthEarth and and presumablypresumably the the wholewhole SolarSolar System System containscontains a a preponderancepreponderance of negative of negative electronselectronsand positive and positive protonsprotons. . ItIt isis quitequite possiblepossible thatthat forforsome of the some of the starsstars itit isis the the otherother way way aboutabout””
DiracDirac Nobel Nobel SpeechSpeech (1933)(1933)
wizard.roma2.infn.it/wizard.roma2.infn.it/pamelapamela
PAMELA
PAMELA Flight Model delivered to Russia,
April 2005AntonovAntonov 72 in Genoa airport72 in Genoa airport
PAMELA onboard during flightPAMELA onboard during flight
Launch preparationLaunch preparationMay 2005 May 2005 –– March 2006 March 2006 TsSKBTsSKB--Progress Progress FactoryFactory
Full qualification testsFull qualification testsMechanical interfacesMechanical interfacesCooling loopCooling loopPower supply testsPower supply testsInterface with VRL Interface with VRL Electrical testsElectrical tests
March 2006 @ March 2006 @ BaykonurBaykonur60 days work before launch60 days work before launch
Standalone testsStandalone testsInsertion into pressurized containerInsertion into pressurized containerElectrical tests with satelliteElectrical tests with satelliteTest of the downlinkTest of the downlink
Distortion on the secondary antiproton flux induced by an ExtragDistortion on the secondary antiproton flux induced by an Extragalactic Antimatter and Black Hole alactic Antimatter and Black Hole evaporation componentsevaporation components
•Background from normal secondary production
•Mass91 data from XXVI ICRC, OG.1.1.21 , 1999
•Caprice94 data from ApJ , 487, 415, 1997
•Caprice98 data from ApJ Letters 534, L177, 2000
Extragalactic AntimatterBlack Hole evaporation
GLAST, PAMELA, LHC, LC Sensitivities to Dark Matter SearchmSUGRA
Sensitivity plot for 5 years observation of mSUGRA for GLAST for tg(b)=55and for other experiments. GLAST 3σsensitivity is shown at the blue line and below for truncated NFW halo profile
accelerator limits @ 100 fb-1 fromH.Baer et al.,hep-ph/0405210
A.Morselli et al, First Glast Symposium, 2007